In this part, we will use the Sen's entropy function formalism [1]} to calculate the conductivities from the information near black hole horizon. By solving the attractor equations, which are derived from the entropy function, one can get the values of the matter fields on the horizon of the black hole without knowing the full solution of the metric. This approach applied in holography was proposed firstly in [2]}, and subsequently in [3]}, [4]}, in which the Maxwell-Dilaton theory and Topological Maxwell theory were discussed respectively. Both of these models were in the framework of classical
Einstein gravity. Here as explained in the introduction, we will consider the holographic model in Gauss-Bonnet gravity to see the effect of stringy correction in the semi-classical limit.
